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Evolution of the Polarization of the Optical Afterglow of the Gamma-Ray

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Evolution of the Polarization of the Optical Afterglow of the Gamma-Ray Evolution of the polarization of the optical afterglow of the gamma-ray burst GRB 030329 Jochen Greiner∗, Sylvio Klose†, Klaus Reinsch‡, Hans Martin Schmidℓ, Re’em Sari$, Di- eter H. Hartmann¶, Chryssa Kouveliotou§, Arne Rau∗, Eliana Palazzi♦, Christian Straubmeier∗∗, Bringfried Stecklum†, Sergej Zharikov††, Gaghik Tovmassian††, Otto B¨arnbantner♯, Christoph Ries♯, Emmanuel Jehin¶¶, Arne Henden§§, Anlaug A. Kaas‡‡, Tommy Grav$$, Jens Hjorthℓℓ, Holger Pedersenℓℓ, Ralph A.M.J. Wijers#, A. Kaufer¶¶, Hye-Sook Park♦♦, Grant Williams♯♯, Olaf Reimer## ∗Max-Planck-Institut f¨ur extraterrestrische Physik, 85741 Garching, Germany †Th¨uringer Landessternwarte, 07778 Tautenburg, Germany ‡Universit¨ats-Sternwarte G¨ottingen, 37083 G¨ottingen, Germany ℓInstitut f¨ur Astronomie, ETH Z¨urich, 8092 Z¨urich, Switzerland $California Institute of Technology, Theoretical Astrophysics 130-33, Pasadena, CA 91125, USA ¶Clemson University, Department of Physics and Astronomy, Clemson, SC 29634, USA §NSSTC, SD-50, 320 Sparkman Drive, Huntsville, AL 35805, USA ♦Istituto di Astrofisica Spaziale e Fisica Cosmica, CNR, Sezione di Bologna, 40129 Bologna, Italy ∗∗ I. Physikalisches Institut, Universit¨at K¨oln, 50937 K¨oln, Germany ††Instituto de Astronomia, UNAM, 22860 Ensenada, Mexico ♯Wendelstein-Observatorium, Universit¨atssternwarte, 81679 M¨unchen, Germany ¶¶European Southern Observatory, Alonso de Cordova 3107, Vitacura, Casilla 19001, Santi- ago 19, Chile §§Universities Space Research Association, U.S. Naval Observatory, P.O. Box 1149, Flagstaff, AZ 86002, USA arXiv:astro-ph/0311282v1 12 Nov 2003 ‡‡Nordic Optical Telescope, 38700 Santa Cruz de La Palma, Spain $$University of Oslo, Institute for Theoretical Astrophysics, 0315 Oslo, Norway, and Harvard- Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA ℓℓAstronomical Observatory, NBIfAFG, University of Copenhagen, 2100 Copenhagen , Den- mark #Astronomical Institute Anton Pannekoek, Kruislaan 403, 1098 SJ Amsterdam, The Nether- lands ♦♦Lawrence Livermore National Laboratory, University of California, P.O. Box 808, Liver- more, CA 94551, USA ♯♯MMT Observatory, University of Arizona, Tucson, AZ 85721, USA ##Theoretische Weltraum-und Astrophysik, Ruhr-Universit¨at Bochum, 44780 Bochum, Ger- many The association of a supernova with GRB 0303291,2 strongly supports the collapsar model3 of γ-ray bursts (GRBs), where a relativistic jet4 forms after 1 the progenitor star collapses. Such jets cannot be spatially resolved because of their cosmological distances. Their existence is conjectured based on breaks in GRB afterglow light curves and the theoretical desire to reduce the GRB energy requirements. Temporal evolution of polarization5,6,7 may provide independent evidence for the jet structure of the relativistic outflow. Small-level polarization (∼1-3%)8−17 has been reported for a few bursts, but the temporal evolution of polarization properties could not be established. Here, we report polarimetric observations of the afterglow of GRB 030329 with high signal-to-noise and high sampling frequency. We establish the polarization light curve, detect sustained polarization at the percent level, and find significant variability. The data im- ply that the afterglow magnetic field has small coherence length and is mostly random, probably generated by turbulence, in contrast with the high polariza- tion detected in the prompt γ-rays from GRB 02120618. Our results suggest a different structure and origin of the magnetic field in the prompt vs. afterglow emission regions. GRB 030329 triggered the High Energy Transient Explorer, HETE-II, on March 29, 2003 (11:37:14.67 UT)19. The discovery of the burst optical afterglow20,21 was quickly followed by a redshift measurement22 for the burster of z=0.1685 (∼800 Mpc), thus making GRB 030329 the second closest long-duration23 GRB ever studied, after GRB 9804253. The proximity of GRB 030329 resulted in very bright prompt and afterglow emission, leading to the best- sampled afterglow to date. Detailed optical spectroscopy revealed an underlying supernova (SN 2003dh)1,2 with an astonishing spectral similarity to SN 1998bw (at z=0.0085, associated with GRB 9804253), thus strongly supporting the link of long-duration GRBs with core- collapse supernovae. The apparent brightness of GRB 030329 also afforded a unique opportunity to study the temporal evolution of polarization in the afterglow phase. Previous single measurements found low-level (1-3 %) polarization8−15 in optical afterglows, and the only reports on vari- able polarization16,17 were based on few measurements with different instruments and modest signal-to-noise. We have overcome the previous sampling limitations with 31 polarimetric ob- servations of the afterglow of GRB 030329 obtained with the same instrumentation (plus few more with different instruments) over a time period of 38 days for a total of an unprecedented ∼50 hours of observations with an 8 m telescope. For the first time we establish a polarization light curve for an optical gamma-ray burst afterglow. We performed relative photometry, and derived from each pair of simultaneous measure- ments at orthogonal angles the Stokes parameters U and Q. In order to obtain the intrinsic polarization of the GRB afterglow, we have to correct for Galactic interstellar polarization (mostly due to dust). We performed imaging polarimetry to derive the polarization parame- ters of seven stars in the field of GRB 030329, and obtained an interstellar (dust) polarization correction of 0.45% at position angle 155deg. Subtraction of the mean foreground polarization was performed in the Q/U plane (Qfp=0.0027±0.0013, Ufp=-0.0033±0.0017). Figure 1 shows an R band image of the GRB 030329 field with the polarization ”vectors” superimposed. The temporal evolution of the degree and angle of polarization together with the R band photometry is shown in Figure 2. This figure demonstrates the presence of non-zero polar- 2 ization, Π ∼0.3-2.5 % throughout a 38-day period, with significant variability in degree and angle on time scales down to hours. Further, the spectropolarimetric data of the first three nights as well as the simultaneous R and K band imaging polarimetry during the second night show that the relative polarization and the position angle are wavelength independent (within the measurement errors of about 0.1 %) over the entire spectral range. These data imply that polarization due to dust in the host galaxy of GRB 030329 does not exceed ∼0.3 %. Dust destruction in the vicinity of the gamma-ray burster due to the strong radiation field would result in a monotonically decreasing polarization degree at constant position angle, which is not observed during the first days. We therefore conclude that the bulk of the observed variability is intrinsic to the afterglow. Figure 2 shows that while the polarization properties show substantial variability (for which no simple empirical relationship is apparent), the R band flux is a sequence of power laws. During each of the power law decay phases the polarization is of order few percent, different from phase to phase, and variable within the phase, but not in tandem with the ”bumps and wiggles” in the light curve. We observe a decreasing polarization degree shortly after the light curve break at ∼0.4 days (as determined from optical21,24 and X-ray data25,26). Rapid variations of polarization occur ∼1.5 days after the burst, and could be related to the end of the transition period towards a new power law phase starting at ∼1.7 days. Polarization eventually rises to a level of ∼2 %, which remains roughly constant for another two weeks. At late time the underlying Type Ic SN 2003dh1,2 increasingly contributes to the total light and probably also to the observed polarization properties. Asymmetries in this type of supernova can produce polarization of order 1 %27,28, as we observe towards the end of our campaign. GRB 030329 belongs to a growing group of bursts for which densely monitored afterglow light curves show significant ”bumps” and ”wiggles” relative to a simple power law decay (most notably GRB 021004 and GRB 011211). These bumps and wiggles complicate the interpretation of the polarization properties. While the rapid decrease in polarization degree during the first night is consistent with the model predictions5,6,7, the position angle changes are not, and thus it remains to be proven whether or not these early polarization data support the break at 0.4 days as due to a jet. A connection to theoretical models throughout the entire period covered in Fig. 2 is a daunting task. A detailed comparison of our data with characteristic features of various theoretical models is beyond the scope of this paper, and will be presented elsewhere. In summary, our data constitute the most complete and dense sampling of the polarization behaviour of a GRB afterglow to date. For GRB 030329 we conclude that the afterglow polarization probably did not rise above ∼2.5 % at any time, and that the polarization did not correlate with the flux. The low level of polarization implies that the components of the magnetic field parallel and perpendicular to the shock do not differ by more than ∼10%, and suggests an entangled magnetic field, probably amplified by turbulence behind shocks, rather than a pre-existing field. This is in contrast with the high level of polarization detected in the prompt γ-rays from GRB 02120618 and suggests a different structure and origin of the magnetic field in the prompt vs. afterglow emission regions. Evolving polarization properties provide a unique diagnostic tool for GRB studies, and the extremely complex light curve of the optical afterglow of GRB 030329 emphasises that measurements should be carried out with high sampling frequency. 3 1. Stanek, K.Z., et al. Spectroscopic discovery of the supernova 2003dh associated with GRB 030329. Astrophys. J. 591, L17-L20 (2003) 2. Hjorth, J., et al. A very energetic supernova associated with the γ-ray burst of 29 March 2003. Nature 423, 847-850 (2003) 3. Woosley, S.E., Eastman, R.G., Schmidt, B.P.
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